Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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Simultaneous measurement of low- and high-mass IMF slopes in 214 star-forming galaxies reveals diversity, weak correlation between ends, and links to stellar mass, star formation rate, and metallicity.
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.
In 37 massive ETGs, the IMF becomes less bottom-heavy with radius, with average α_IMF falling from 2.16 to 1.74 and IMF gradients dominating M/L variations over stellar population effects.
Bayesian analysis of 163 open clusters finds a universal initial IMF slope of -2.29 with 0.17 scatter and minimal primordial mass segregation, followed by rapid internal mass segregation and later tidal MF flattening.
The paper identifies underproduction of oxygen in low-mass simulated dwarf galaxies as the likely cause of missing OVI in the CGM, based on comparisons across two simulation suites.
Rotating massive-star yields at 300 km/s improve agreement with metal-poor Sc, Ti, V abundances in one-zone GCE models, with IMF slope variations providing secondary modulation.
citing papers explorer
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The impact of stellar binaries and star cluster dynamics on pair-instability supernovae
Binary interactions and cluster dynamics boost PISN rates by up to 3x versus single stars, enabling constraints on stellar-wind mass loss and galaxy metallicity distributions.
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Gauging the Impact of Cosmic Ray Feedback on the Stellar Initial Mass Function
Cosmic ray transport in molecular cloud simulations boosts star formation efficiency by up to 43% and yields a top-heavier IMF with a high-mass slope shallower by ~20%.